Migration and Final Location of Hot Super Earths in the Presence of Gas Giants

Authors: Ji-Lin Zhou, Douglas N.C. Lin

(Submitted on 1 Feb 2008)

Abstract: Based on the conventional sequential-accretion paradigm, we have proposed that, during the migration of first-born gas giants outside the orbits of planetary embryos, super Earth planets will form inside the 2:1 resonance location by sweeping of mean motion resonances (Zhou et al. 2005). In this paper, we study the subsequent evolution of a super Earth (m_1) under the effects of tidal dissipation and perturbation from a first-born gas giant (m_2) in an outside orbit. Secular perturbation and mean motion resonances (especially 2:1 and 5:2 resonances) between m_1 and m_2 excite the eccentricity of m_1, which causes the migration of m_1 and results in a hot super Earth. The calculated final location of the hot super Earth is independent of the tidal energy dissipation factor Q’. The study of migration history of a Hot Super Earth is useful to reveal its Q’ value and to predict its final location in the presence of one or more hot gas giants. When this investigation is applied to the GJ876 system, it correctly reproduces the observed location of GJ876d around 0.02AU.

Comments: 7 pages, 4 figures

Subjects: Astrophysics (astro-ph)

Journal reference: IAU Symposium 249: Exoplanets: Detection, Formation and Dynamics. Y.-S. Sun, S. Ferraz-Mello & J.-L. Zhou (eds.), 2008, p285-291
Cite as: arXiv:0802.0062v1 [astro-ph]

Submission history

From: Ji-Lin Zhou [view email]

[v1] Fri, 1 Feb 2008 07:09:50 GMT (289kb)

http://arxiv.org/abs/0802.0062

H2O and OH gas in the terrestrial planet-forming zones of protoplanetary disks

Authors: C. Salyk, K.M. Pontoppidan, G.A. Blake, F. Lahuis, E.F. van Dishoeck, N.J. Evans II

(Submitted on 1 Feb 2008)

Abstract: We present detections of numerous 10-20 micron H2O emission lines from two protoplanetary disks around the T Tauri stars AS 205A and DR Tau, obtained using the InfraRed Spectrograph on the Spitzer Space Telescope. Follow-up 3-5 micron Keck-NIRSPEC data confirm the presence of abundant water and spectrally resolve the lines. We also detect the P4.5 (2.934 micron) and P9.5 (3.179 micron) doublets of OH and 12CO/13CO v=1-0 emission in both sources. Line shapes and LTE models suggest that the emission from all three molecules originates between ~0.5 and 5 AU, and so will provide a new window for understanding the chemical environment during terrestrial planet formation. LTE models also imply significant columns of H2O and OH in the inner disk atmospheres, suggesting physical transport of volatile ices either vertically or radially; while the significant radial extent of the emission stresses the importance of a more complete understanding of non-thermal excitation processes.

Comments: 9 pages, 3 figures, 1 table, aastex, to appear in the Astrophysical Journal

Subjects: Astrophysics (astro-ph)

Cite as: arXiv:0802.0037v1 [astro-ph]

Submission history

From: Colette Salyk [view email]

[v1] Fri, 1 Feb 2008 00:01:00 GMT (183kb)

http://arxiv.org/abs/0802.0037